研究生: |
羅經閔 Ching-Min Lo |
---|---|
論文名稱: |
利用UKIDSS-UDS資料來統計紅移1到3之間的紫外線光度密度 UKIDSS-UDS: UV-Luminosity density at 1<z<3 |
指導教授: |
傅谷石
Sebastien Foucaud |
學位類別: |
碩士 Master |
系所名稱: |
地球科學系 Department of Earth Sciences |
論文出版年: | 2013 |
畢業學年度: | 101 |
語文別: | 英文 |
論文頁數: | 51 |
中文關鍵詞: | star-forming galaxy 、star-formation rate 、star formation history |
英文關鍵詞: | star-forming galaxy, star-formation rate, star formation history |
論文種類: | 學術論文 |
相關次數: | 點閱:168 下載:1 |
分享至: |
查詢本校圖書館目錄 查詢臺灣博碩士論文知識加值系統 勘誤回報 |
The star formation history is a key-element to understand galaxy evolution and formation. Recent studies have shown that the star-formation rate peaks at redshift z=1-3 and then decline to its local value. The physical processes responsible for the sudden quenching of star-formation are still unknown. In order to better understand the origin of these effects, we propose in this study to use the UV-luminosity as an indicator of the Star-formation rate. We take advantage of our deep NIR/optical data from the UKIDSS-UDS/SXDS survey and our very deep CFHT U-band data to compute the luminosity function of galaxies at z=1-3. Then we fit a Schechter function and integrate to compute the luminosity density to explore the evolution of the star-formation rate.
The star formation history is a key-element to understand galaxy evolution and formation. Recent studies have shown that the star-formation rate peaks at redshift z=1-3 and then decline to its local value. The physical processes responsible for the sudden quenching of star-formation are still unknown. In order to better understand the origin of these effects, we propose in this study to use the UV-luminosity as an indicator of the Star-formation rate. We take advantage of our deep NIR/optical data from the UKIDSS-UDS/SXDS survey and our very deep CFHT U-band data to compute the luminosity function of galaxies at z=1-3. Then we fit a Schechter function and integrate to compute the luminosity density to explore the evolution of the star-formation rate.
Arnouts et al. 1999, MNRAS, 310, 540
Bertin & Arnouts 1996, A&A Supplement, 317, 393
Blanton et al. 2003a, AJ, 125, 2348
Bouwens et al. 2007, ApJ, 670, 928
Caputi et al. 2007, ApJ, 660, 97
Coleman et al. 1980, ApJS, 43, 393
Cowie et al. 1996, AJ, 112, 839
Cucciati et al. 2012, A&A, 539, A31
Dekel & Birnboim 2006, MNRAS, 368, 2
Erb et al. 2006c, ApJ, 646, 107
Faber et al. 2007, ApJ, 665, 265
Fan et al. 2001, AJ, 122, 2833
Furusawa et al. 2008, ApJS, 176, 1
Gilli et al. 2007, A&A, 463, 79
Granato et al. 2004, ApJ, 600, 580
Hartley et al. (in prep)
Hirashita et al. 2003, A&A, 410, 83
Hopkins et al. 2006, ApJ, 652, 107
Hopkins et al. 2007, ApJ, 654, 731
Ilbert et al. 2004, MNRAS, 351, 541
Ilbert et al. 2005, A&A, 439, 863
Kinney et al. 1996, ApJ, 467, 38
Kriek et al. 2006, ApJ, 649L, 71
Lawrence et al. 2007, MNRAS, 379 ,1599
Lehmer et al. 2008, ApJ, 681, 1163
Lilly et al. 1995, ApJ, 455, 108
Marshall 1985, ApJ, 289, 457
Norman et al. 2004, ApJ, 607, 721
Oesch et al. 2010, APJ, 725, 150
Oke, J.B. 1974, ApJS, 27, 21
Perez-Gonzalez et al. 2005, ApJ, 630, 82
Quadri et al. 2012, ApJ, 744, 88
Reddy et al. 2008, ApJS ,175, 48
Sawicki et al. 2005, ApJ, 635, 100
Sawicki et al. 2006, ApJ, 642, 653
Scannapieco et al. 2005, ApJ, 635, 13
Schechter 1976, ApJ, 203, 297
Schiminovich et al. 2005, ApJ, 619, 47
Shaver et al. 1996, Nature, 384, 439
Simpson et al., 2012, MNRAS, 421, 3060
Steidel et al. 2004, ApJ, 604, 534
Swindle et al. 2011, AJ, 142, 118
Tresse et al. 2002, MNRAS, 337, 369
Tresse et al. 2007, A&A, 472, 403
Zucca et al. 2006, A&A, 455, 879